A&G • February 2013 • Vol. 54 1.25 The continuous flow of matter that escapes out of the solar gravitational well is known as the solar wind. As the material flows out of the Sun, it is accelerated to between 400 and 800 km s. Through this continuous flow of material, the Sun loses more than one million tonnes every second. But this is just a tiny fraction, corresponding to 2 × 10 of a solar ma...

Fast solar wind has been recognized, about 40 years ago, to originate in polar coronal holes (CHs), that, since then, have been identified with sources of recurrent high speed wind streams. As of today, however, there is no general consensus about whether there are, within CHs, preferential locations where the solar wind is accelerated. Knowledge of slow wind sources is far from complete as wel...

The abundance of He in the present day local interstellar cloud (LIC) and in the sun has important implications for the study of galactic evolution and for estimating the production of light nuclei in the early universe. Data from the Solar Wind Ion Composition Spectrometer (SWICS) on Ulysses is used to measure the isotopic ratio of helium (He=He = Γ) both in the solar wind and the local inters...

[1] On 17 September 2000 the IMF was directed continuously northward for more than 3 hours. Density fluctuations in the solar wind resulted in quasiperiodic variations in the solar wind dynamic pressure, and correlated fluctuations also occurred in the IMF Bz component. The Northern Hemisphere SuperDARN radars observed bursts of highlatitude high-velocity plasma flow during this northward IMF i...

A&G • February 2013 • Vol. 54 1.25 The continuous flow of matter that escapes out of the solar gravitational well is known as the solar wind. As the material flows out of the Sun, it is accelerated to between 400 and 800 km s. Through this continuous flow of material, the Sun loses more than one million tonnes every second. But this is just a tiny fraction, corresponding to 2 × 10 of a solar ma...

A&G • February 2013 • Vol. 54 1.25 The continuous flow of matter that escapes out of the solar gravitational well is known as the solar wind. As the material flows out of the Sun, it is accelerated to between 400 and 800 km s. Through this continuous flow of material, the Sun loses more than one million tonnes every second. But this is just a tiny fraction, corresponding to 2 × 10 of a solar ma...

The Western Wind and Solar Integration Study Phase 1 (WWSIS1) investigated the impacts of high penetrations of wind and solar power on the Western Interconnection of the United States. The Western Wind and Solar Integration Study Phase 2 (WWSIS2) built on Phase 1 but with far greater refinement in the level of data inputs and production simulation. It considered the differences between wind and...

Voyager 2 and Ulysses were at nearly the same latitude in the southern heliosphere at the beginning of 1999 and their radial separation was about 55 AU. The e ect of pickup ions should be profound at Voyager's position, especially, the deceleration of the solar wind ow. This unique opportunity allows us to investigate the e ect of pickup ions based on direct multi-spacecraft observations. The U...

[1] A discrete set of climatological patterns of high‐latitude ionospheric convection are derived using line‐of‐sight plasma drift data from the Super Dual Auroral Radar Network (SuperDARN). The patterns are derived independently for the Northern Hemisphere and Southern Hemisphere and for varying solar wind, interplanetary magnetic field (IMF), and dipole tilt angle conditions. By interpolating...